52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1182.pdf

SuperCam on the Perseverance Rover for Exploration of Crater: Remote LIBS, VISIR, Raman, and Time-Resolved Luminescence Spectroscopies Plus Micro-Imaging and Acoustics R.C. Wiens1, S. Maurice2, O. Gasnault2, R.B. Anderson3, O. Beyssac4, L. Bonal5, S. Clegg1, L. Deflores6, G. Dromart7, W.W. Fischer8, O. Forni2, J.P. Grotzinger8, J.R. Johnson9, J. Martinez-Frias10, N. Mangold11, S. McLennan12, F. Montmessin13, F. Rull14, S.K. Sharma15, A. Cousin2, P. Pilleri2, V. Sautter16, E. Lewin17, E. Cloutis18, F. Poulet19, S. Bernard16, T. McConnochie20, N. Lanza1, H. Newsom21, A. Ollila1, R. Leveille22, S. Le Mouelic11, J. Lasue2, N. Melikechi23, P.-Y. Meslin2, O. Grasset11, S.M. Angel24, T. Fouchet25, P. Beck17, B. Bousquet26, C. Fabre27, P. Pinet2, K. Benzerara4, G. Montagnac7, G. Arana28, K. Castro28, J. Laserna29, J.M. Madariaga28, J.-A. Manrique14, G. Lopez14, R. Lorenz9, D. Mimoun30, T. Acosta-Maeda15, C. Alvarez29, E. Dehouck31, G. Delory, A. Doressoundiram25, R. Francis6, J. Frydenvang32, T. Gabriel3, X. Jacob30, M.B. Madsen32, J. Moros29, N. Murdoch30, R. Newell1, J. Porter15 C. Quantin-Nataf31, W. Rapin2, S. Schröder33, P. Sobron34, M. Toplis2, A.J. Brown35, M. Veneranda14, B. Chide2, C. Legett1, C. Royer19, A. Stott30, D. Vogt33, S. Robinson1, D. Delapp1, E. Clavé26, S. Connell18, A. Essunfeld1, Z. Gallegos21, C. Garcia-Florentino28, E. Gibbons22, J. Huidobro28, E. Kelly15, H. Kalucha8, P. Ruiz28, I. Torre- Fdez28, S. Shkolyar20, and the SuperCam Team (1LANL, Los Alamos, NM; [email protected], 2IRAP, Toulouse, ; 3USGS; 4IMPMC; 5IPAG; 6JPL; 7PGLTPE; 8Caltech; 9APL/JHU; 10CSIC-UCM; 11LPG Nantes; 12Stonybrook; 13LATMOS; 14UVa-CSIC; 15U. Hawaii; 16MNHN; 17U. Grenoble; 18U. Winnipeg; 19IAS, U-Paris Saclay; 20GSFC; 21UNM; 22McGill; 23U Mass Lowell; 24USC; 25LESIA; 26LAB; 27U. Nancy; 28UPV-EHU; 29U. Malaga; 30ISAE-SUPAERO; 31U. Lyon; 32U. Copenhagen; 33DLR; 34SETI; 35Plancius Research)

Introduction: NASA’s Perseverance rover carries 7 instruments and a Sample Cache Sys- tem. This mission has 4 major goals: a) explore an astrobiologically relevant ancient environment, b) assess bio-signature preservation potential, c) cache samples for eventual return to Earth, and d) advance technologies for human exploration [1]. SuperCam provides a wide range of remote ob- servations to support the first 3 goals. Here we describe SuperCam’s capabilities as shown prior to launch; presentation at the meeting may report the status a month after landing at Jezero crater.

Instrument Description: SuperCam uses re- mote laser-induced breakdown spectroscopy (LIBS) to obtain quantitative elemental composi- tions to 7 m and provides high-resolution images of the targets, like its predecessor [2, 3]. Co- boresighted with the LIBS, SuperCam returns mineralogy via a combination of remote time- resolved Raman (to ~7 m) and visible and infra- red (VISIR) reflectance spectroscopy (any dis- tance). The LIBS shock wave removes dust for all spectral techniques, giving access to the targets’ surfaces. The hardware built for Raman spectros- copy also allows time-resolved luminescence (TRL) spectroscopy, which remotely provides signals from rare-earth elements (REEs) [4, 5]. Passive spectroscopy can also be used to study atmospheric gases, ice, and dust [6]. Finally, Su- perCam performs acoustic spectral sensing to study phenomena [10] and to be used with the LIBS shock waves to study the physical prop- erties of the targets [7-9]. SuperCam follows ChemCam’s architecture [2, 3], consisting of two separate units—one on the rover’s mast and one in the body—as well as a set of calibration targets (Fig. 1). The Mast Unit (MU) contains a Nd:YAG pulsed laser, a 104 mm dia. telescope, a wavelength-scanning infrared spectrometer (1.3-2.6 µm, 256 channels), a high- Fig. 1. SuperCam Mast Unit (a), Body Unit (b), resolution Remote Micro-Imager (RMI; 2k x 2k and Calibration Target Assembly (c). Long dimen- CMOS with Bayer filter), and a (100 sions of each unit are 383, 221, and 110 mm, re- to 20k Hz) [11]. spectively. 52nd Lunar and Planetary Science Conference 2021SuperCam (LPI onContrib the Perseverance. No. 2548 Rover) 1182.pdf

Light collected by the telescope in the 245- Acoustic testing was carried out with the Mi- 855 nm range is sent via a 6 m optical fiber from crophone at various stages including near the mast to the Body Unit (BU), which contains pressure on the rover during STT, when a meas- three optical spectrometers. The UV (245-340 urement of the speed of sound was obtained [19]. nm) and violet (385-465 nm) spectrometers are Initial microphone observations should be able to replicas of ChemCam’s, while the third one (535- resolve long-standing questions about frequency- 855 nm; 110-7100 cm-1) is a high-efficiency dependent attenuation of sound waves in the transmission spectrometer containing a time- Mars atmosphere. A separate presentation on gated (to 100 ns) optical intensifier, enabling the acoustics will be given at this meeting [20]. time-resolved Raman and luminescence meas- A separate presentation on atmospheric obser- urements, as well as the LIBS and passive visible- vation capabilities will also be given at this meet- range spectroscopy [12]. An expanded set of cali- ing [21]. bration targets are mounted at ~1.55 m distance SuperCam Initial Checkout on Mars: If the on the back of the rover [13]. These targets were landing is successful, health checks are planned selected with Jezero crater in mind, including before and after deployment of the rover’s mast carbonates, serpentine, and olivine. and installation of surface software in the first Pre-Launch Performance: Tests were per- week on the surface. Initial observations will be formed at the integrated instrument level and on done by the RMI and passive techniques to verify the rover to calibrate [23] and demonstrate its proper commanding of the mast position prior to capabilities. LIBS performance is expected to use of the laser-based techniques. Initial observa- meet or exceed that of ChemCam. Some spectral tions will concentrate on the onboard targets to regions have higher resolution and the intensifier establish initial calibrations (wavelength, focus, allows some new tests for time-resolved LIBS white reference target for VISIR, and eventually [12]. The LIBS laser beam has slightly smaller compositional calibrations for LIBS); initial diameter at best focus, e.g., 200-450 µm [11]. sound recordings and spectral rasters on the Mars LIBS performance is highlighted in a separate surface in the first several weeks will test opera- presentation [14]. tional sequences. Science targets should become Time-resolved tests at interleaved with checkouts as time progresses. various distances ≥ 2 m [12] showed observation First results may be reported at the meeting. of peaks identifying various minerals. They in- References: [1] Mustard J.F. et al. (2013) cluded minerals of astrobiological interest due to Science Definition Team report. Farley K. et al. their high preservation potential on Earth [22], (2021), this meeting. [2] Wiens R.C. et al. (2012) such as carbonates (calcite, dolomite, magnesite, SSR 170, 167. [3] Maurice S. et al. (2012) SSR siderite, ankerite) and sulfates. Other observed 170, 95. [4] Gaft M. et al. (2015) Modern Lumi- minerals included phosphates, fluorite, apophyl- nescence Spectroscopy of Minerals and Materi- lite, and various silicates (olivine, quartz, diop- als, Springer. [5] Ollila A.M. et al. (2018) LPSC side, labradorite, microcline, oligoclase). Studies 49, 2786. [6] McConnochie T.H. et al. (2017) were also made of organic mixtures [15]. Grain- Icarus.2017.10.043. [7] Murdoch N. et al. (2018) size studies indicate that performance will be best PSS 165, 260. [8] Chide B. et al. (2020) Spectro- on medium to coarse sand on the Wentworth chim. Acta B 153, 50. [9] Chide B. et al. (2020) scale. Remote TRL studies showed the presence Spectrochim. Acta B 174, 106000. [10] Chide B. of Sm, Nd, Eu, and other REEs in REE-rich min- et al. (2021) Icarus 354, 114060. [11] Maurice S. eral grains (e.g., apatite, zircon). Raman and TRL et al. (2020) SSR, SPAC-D-20-00069R1. [12] performance is highlighted in a separate presenta- Wiens R.C. et al. (2020) SSR 10.1007/s11214- tion [15]. Separate studies at this meeting high- 020-00777-5. Fouchet. T. et al. (2021), submitted. light LIBS-Raman synergies on carbonates, ob- [13] Manrique J.-A. et al. (2020) SSR 216, 138. served in the laboratory [24]. Cousin A et al. (2021) in preparation. [14] Ander- The SuperCam IR spectrometer was calibrated son R.B. et al., this meeting. [15] Beyssac O. et prior to integration with the instrument [16]. Test- al., this meeting. [16] Royer C. et al. (2020) RSI ing of the VISIR systems at the integrated level 91, 063105. [17] Fouchet T. et al., this meeting. was confined to the rover system thermal test [18] Gasnault O. et al. (2021), this meeting. [19] (STT) due to the need for the spectrometer to be Chide B. et al. (2020) LPSC 51, 1366. [20] Chide cold. During that test, observations of the rover B. et al., this meeting. [21] McConnochie T. et calibration targets and other mineral targets al., this meeting. [22] Farmer J.D. and DesMarais demonstrated excellent performance comparable D.J. (1999) JGRP 104, 26977. [23] Legett C. et to laboratory instruments [12]. VISIR perfor- al. (2021) this meeting. [24] Clavé E. et al., this mance is highlighted in a separate presentation at meeting; Veneranda M. et al., this meeting. this meeting [17]. Imaging tests with SuperCam’s RMI were car- ried out largely prior to instrument integration, showing its 18.8 mrad field of view and ~80 µrad resolution, limited by the telescope design rather than pixels [11]. A separate presentation shows the RMI’s performance [18].